... The flag selections are read from the DSS keywords of the input image. ... The following filters are read from the data subspace keywords of the input images and are taken into account for the calculation of the exposure maps: TIME range filters, GTI filters, CCDNR range filters, FLAG range filters, FLAG bit-mask filters. If parameter usedss is set to false, the task tries to determine the exposure time by looking for gti extensions in the input image of the form STDGTInn, STDGTIn, STDGT, or GTI. ...

... The models provided are: . abs - absorption of x-rays by neutral gas with solar abundances. parameter 1 = . ... parameter 2 = . ... normalization - logarithmic value of the flux density at 1 keV in units of keV cm -2 s -1 keV -1 . ... normalization - logarithmic value of the normalization of the gaussian in units of keV cm -2 s -1 . ... absorption ( params )* model ( params ) . ... A single value for the normalization (i.e., fixed normalization) will force the program to use that value. ...

... Figure: Massive binary evolutionary track. ... A short glance to this track is sufficient to understand that there are a lot of evolutionary scenario parameters, which affect different stages of the binary evolution. Fortunately, a very limited number of parameters has effect on the compact binary merging rate. ... The most important (and practically unique) parameter changing the galactic binary NS merging rate is the distribution of an additional (kick) velocity imparted to NS at birth. ...

... We present a computer program for modelling energy flux distribution and light curves of eclipsing binaries from far ultraviolet to infrared regions. The Roche model is assumed. Proximity effects of components (reflection of radiation and surface gravity darkening) are taken into account. ... Figure 1: The surface temperature distribution for Algol A-B system before (upper plot) and after (lower plot) correction for temperature due to the irradiation effect. ...

Next: Summary of reduction Up: Echelle Reduction Previous: Saving the Data . In the present version we will be concerned with the standard configuration of CASPEC, the Cassegrain Echelle Spectrograph which is in operation at the Cassegrain focus of the ESO 3.6 m telescope. ... In its standard configuration CASPEC uses a a 31.6 lines/mm echelle grating together with a 300 lines/mm grating cross disperser. ... The table shows the change in resolution with the order number. Table: Resolution . ...

... CentralProcessor 0.11 documentation . ... It can be run with the following command, where ?config.in? is a file containing the configuration parameters described in the next section. ... Parset parameters understood by ccontsubtract are given in the following table (all parameters must have CContSubtract prefix, i.e. CContSubtract.dataset ). ... A number of other parameters allowing the user to narrow down the data selection are understood. ... Parameter . ... Data set file name to work with. ...

... SFIT is a general-purpose code designed to optimize theoretical stellar spectra to an observed spectrum. ... While the programme expects input from "stdio", it is more natural to save commands in a file (eg "sfit_input") and run the code simply by . ... If the spectra to be fitted have a filename "star_spectrum", then the best fit spectrum will be written out, together with the renormalized input spectrum, to a file called "star_spectrum.fit". ... sets up model spectrum grid (and for 2nd star) . ...

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

AO Home AO Astronomy Robert Minchin Blog Publications IDL Routines . Rotang can either be run from the command line as described here or through the alfa_ang GUI . ... To run rotang at Arecibo: . Start IDL . ... Run Rotang: . rotang, Date , RA , Dec , Time , /choice . ... Rotang also calculates the Azimuth and Zenith Angle fir every source. If the Zenith Angle is greater than 20 degrees, then the program will return that the source is down and will not calculate an optimum ALFA angle. ...

The determination of the detector parameters is based on sets of images of a spatially uniform-illumination scene (flatfield frames) and without any illumination (dark frames), putting a plug in place of the filter, taken at a series of exposure times. ... We interleave before and after each exposure time in the series of flatfield frames a set of reference images at an exposure time of 1 sec to determine the possible temporal variation of the illumination level. ...

... There are a lot of computer codes simulating this scattering and freely available in the Internet (see e.g. links on our JPDOC page ). ... The code and input file are available in the directory . ... A slightly modified code of Barber Hill with a C-shell and input files is available in the directory . ... The code, input and test output files are available in the directory . ... See also readme file. file. ... The code, input file and their description (a TeX file) are available in the directory . ...

... Column (1): Source name from NED. ... Column (8): Log star formation rate, from SDSS. {\it Detected sources:} (1) (2) (3) (4) (5) (6) (7) IC0159 0.58±0.10 8.31 ± 0.07 8.25 ± 0.07 9.55 9.70 8.89 -0.06 UGC2004 5.98±0.65 9.32 ± 0.04 9.03 ± 0.04 9.83 9.61 9.15 0.36 NGC1234 0.24±0.06 7.92 ± 0.09 7.80 ± 0.09 9.67 9.58 8.98 -0.68 2MASJ0839+03 2.30±0.54 8.91 ± 0.09 8.69 ± 0.09 --- 9.94 9.08 0.58 2MASJ0846+02 2.75±0.47 8.98 ± 0.07 8.85 ± 0.07 --- 9.84 8.99 ...

Table 4.1: Solar System Standard Targets . Table 4.2: Target Description Keywords . Table 4.3: Positional Parameters for TYPE = COMET . ... Observers for solar system Targets of Opportunity (e.g. a "new" comet or asteroid, a solar-wind disturbance reaching the Jovian magnetosphere, etc.), should complete the Generic Target List ( See 3.12 Generic Targets List [Generic_Targets] ) and the Visit and Exposure Specifications (to the extent possible) in time for the Phase II deadline. ...

Stellarium 0.12.3 . ... TextParams Struct Reference . Parameters specifying how to draw text. ... TextParams (const float x, const float y, const QString &string) . Construct TextParams with default parameters. ... TextParams ( Vector3 < F > &position3D, StelProjectorP projector , const QString &string) . Construct TextParams to draw text at a 3D position, using specified projector. ... string љ . ... Text string to draw. ... The required string parameter is also set, as is the projector. ...

... Публикации и издания Публикации профессорско-преподавательского состава СГАУ Издания проф. Сосниной Т.Н. Biosphere: Analysis of Value Parameters . ... Besides, the ways of saving the use value and value properties of biosphere are analyzed. The expediency of transformation of two-criterion theory of value into the three- criterion theory of the balance of value, where the ecologic component performs the function of the key criterion has been founded. ... BIOSPHERE USE VALUE OF THE PRODUCT: MAIN . ...

... Co-ordinate systems description . Directories structure . The file names' construction . The file set description . ... The orbital information for each month is presented in the separate directory. The INTERBALL orbital data are located on the STDA server, for each month in the separate subdirectory, which name consists from the year (YYYY) and month (MM) numbers. The Parent Directory of the Tail Probe orbital data is http://www.iki.rssi.ru/da/interball/tail/orbit/ . ...

Orbital data : INTERBALL AZ GSE and GSM cartesian coordinates, GSE cartesian velocity (once per 10 minutes). ... Magnetic field data from IMAP experiment. Magnetic fileld absolute value and magnetic field index (the difference between absolute value and model value), status flag. ... Counts of H+ and O+ ions are accumulated during one spin period by detectors D6 (antisunward looking), D8 (spin plane), D10 (sunward looking) of TRICS2 subsystem (1.0-30 keV). ... TRICS1, TRICS2, TRICS3 subsystems: . ...

... Exposure Time Calculator (ETC) . ... ESO - Public Surveys . ... the recommended values to use for DIT, . ... Detector on-chip integration (DIT): seconds. to your chosen value - a separate page gives recommended values to use for DIT - for modes 1 and 2 below you may wish to start with the maximum recommended values as these will minimize the effect of read noise (a total object exposure of Y secs with DIT=X secs will produce Y/X lots of read noise) and give you a lower limit on the time needed. ...

... FTP access the basic models is here . ... Below, we put short descriptions of the used SED models for the photometric redshifts providing by the current server . ... The uniqueness of this model consists in expanding to the near IR (NIR) of Rocca-Volmerange and Guiderdoni's (1988) atlas of synthetic spectra with a revised stellar library, which includes parameters of cool stars. ... Homepage of the GISSEL model). ... Another model used earlier is the model of synthetic spectra of Poggianti (1997). ...